Thus we use a model including a disc to produce the soft X-ray
component, thermal Comptonisation of these disc seed photons to
produce the hard continuum, and reflection of the hard continuum from
the surface of the disc. We use the thcomp model to describe the
Comptonisation, developed and tested by [1]}, extended to include its reflected continuum and
self-consistent line emission by [2]}. We assume
that the reflecting material is neutral, with solar abundances and
inclined at \(60^\circ \) . We fix the galactic absorption column at
\(N_H=0.2\times 10^{22}\)  cm\(^{-2}\)  corresponding to an \(E(B-V)=0.34\) 
[3]}. The results for each spectrum are detailed in Table 1.
We assess the significance of the detected disc emission by removing
the disc from the model, and fixing the seed photon temperature
instead at 0.1 eV. This results in a loss of 2 degrees of freedom, so
the disc is only significant at greater than 99 per cent confidence
for \(\Delta \chi ^2 > 4.61\) . Thus all the spectra apart from the final
3 (26, 30 and 31) strongly require the presence of an additional soft
component. We similarly assess the significance of reflection (driven
mostly by the presence of the iron line) and find that it is required
in all the datasets apart from the final 3.
